The sensitivity of the Laser Interferometer Gravitational Wave Observatory ( LIGO ) to a stochastic background , and its dependence on the detector orientations
The sensitivity of the Laser Interferometer Gravitational Wave Observatory ( LIGO ) to a stochastic background , and its dependence on the detector orientations
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激光干涉引力波天文台（LIGO）对随机背景的灵敏度及其对探测器方向的依赖性
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发表时间：
1993
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通讯作者：
Eanna E. Flanagan
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作者：
Eanna E. Flanagan
波动观测站 (LIGO) 的随机背景及其对探测器方向的依赖性。我们分析了干涉仪引力波探测器网络对引力波随机背景的灵敏度，并推导出该灵敏度对探测器臂方向的依赖性。我们以克里斯滕森最近的工作为基础并进行了扩展，但是我们对一对探测器方向的最佳选择的结论与他的不同。对于一对与地心所成角度 < ∼ 70 • 的探测器（例如 LIGO），我们发现最佳配置是每个探测器的臂与连接它们的大圆弧形成 45 •（模 90 •）的角度。对于距离较远的探测器，每个探测器应该有一个臂与该弧线对齐。我们表明，距离 < ∼ 3000 km 的探测器对的随机背景的宽带灵敏度本质上是由它们的相对旋转决定的。它们相对于连接它们的弧线的平均旋转并不重要。我们还详细描述了使用检测器网络搜索随机背景的最佳数据分析算法，该算法隐含在迈克尔逊的早期工作中。 LIGO 探测器对相距约 3000 公里。这些探测器当前规划的方向的最小可检测随机能量密度比最佳方向时的值大 ∼ 3%，并且是它们的间隔 < ∼ 几公里时的 ∼ 4 倍。 [选择探测器 1 相距较远，以便它们的噪声源不相关，并提高确定突发源位置的角分辨率。]
Wave Observatory (LIGO) to a stochastic background, and its dependence on the detector orientations. We analyze the sensitivity of a network of interferometer gravitational-wave detectors to the gravitational-wave stochastic background, and derive the dependence of this sensitivity on the orientations of the detector arms. We build on and extend the recent work of Christensen, but our conclusion for the optimal choice of orienta-tions of a pair of detectors differs from his. For a pair of detectors (such as LIGO) that subtends an angle at the center of the earth of < ∼ 70 • , we find that the optimal configuration is for each detector to have its arms make an angle of 45 • (modulo 90 •) with the arc of the great circle that joins them. For detectors that are farther separated , each detector should instead have one arm aligned with this arc. We show that the broadband sensitivity to the stochastic background of a detector pair which are < ∼ 3000 km apart is essentially determined by their relative rotation. Their average rotation with respect to the arc joining them is unimportant. We also describe in detail the optimal data-analysis algorithm for searching for the stochastic background with a detector network, which is implicit in earlier work of Michelson. The LIGO pair of detectors will be separated by ∼ 3000 km. The minimum detectable stochastic energy-density for these detectors with their currently planned orientations is ∼ 3% greater than what it would be if the orientations were optimal, and ∼ 4 times what it would be if their separation were < ∼ a few kilometers. [The detectors are chosen 1 to be far apart so that their sources of noise will be uncorrelated, and in order to improve the angular resolution of the determinations of positions of burst sources.]